Results from PAMELA, ATIC and FERMI: Pulsars or dark matter?

Chowdhury, Debtosh; Vempati, Sudhir K.; Jog, Chanda J.

doi:10.1007/s12043-011-0019-1

Cited by 8 publications

(6 citation statements)

References 173 publications

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“…For this new dark matter structures, it is hope that other present or the future observations can have the power to give new constraints on them. For the recent observations of positron, such as PAMELA [38], Fermi [39] and ATIC [40], may be the signal from the dark matter annihilation (for a review one can see [41]). The characteristic of UCMHs would explain these observations.…”

Section: Resultsmentioning

confidence: 99%

Constraints on ultracompact minihalos from extragalactic γ-ray background

Yang¹,

Liu²,

Huang³

et al. 2011

J. Cosmol. Astropart. Phys.

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It has been proposed that ultracompact minihalos (UCMHs) might be formed in earlier epoch. If dark matter is in the form of Weakly Interacting Massive Particles (WIMPs), UCMHs can be treated as the γ-ray sources because of the dark matter annihilation within them. In this paper, we investigate the contributions of UCMHs formed during three phase transitions (electroweak symmetry breaking, QCD confinement and e + e − annihilation) to the extragalactic γ-ray background. Moreover, we use the Fermi-LAT observation data of the extragalactic γ-ray background to get the constraints on the current abundance of UCMHs produced during phase transitions. We also compare these results with those obtained from Cosmic Microwave Background (CMB) observations finding that the constraints from the Fermi-LAT are more stringent than CMB.

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Section: Resultsmentioning

confidence: 99%

Constraints on ultracompact minihalos from extragalactic γ-ray background

Yang¹,

Liu²,

Huang³

et al. 2011

J. Cosmol. Astropart. Phys.

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“…That is to say both the astrophysical scenario and DM scenario can give comparable fit to the e þ e À data. We may not be able to discriminate these two scenarios from the e þ e À spectra [36,[64][65][66][67], but need to resort to other probes such as the e þ e À anisotropy [68] and -rays [69].…”

Section: Dark Matter Annihilation Scenariomentioning

confidence: 99%

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

Liu

Yuan

et al. 2012

Phys. Rev. D

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Recently, the PAMELA collaboration published the cosmic nuclei and electron spectra with high precision, together with the cosmic antiproton data updated, and the Fermi-LAT collaboration also updated the measurement of the total e þ e À spectrum to lower energies. In this paper we develop a Markov Chain Monte Carlo (MCMC) package CosRayMC, based on the Galactic Propagation (GALPROP) cosmic ray propagation model to study the implications of these new data. It is found that if only the background electrons and secondary positrons are considered, the fit is very bad with 2 red % 3:39. Taking into account the extra e þ e À sources of pulsars or dark matter annihilation we can give much better fit to these data, with the minimum 2 red % 1:04. This means the extra sources are necessary with a very high significance in order to fit the data. However, the data show little difference between pulsar and dark matter scenarios. Both the background and extra source parameters are well constrained with this MCMC method. The antiproton data can further constrain the branching ratio of dark matter annihilation into quarks to be B q < 0:5% at 2 confidence level. The possible systematical uncertainties of the present study are discussed.

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“…Thus, it is meaningful and significant for us to study the problem again, using Xenon detectors (XEON100 [31], XMASS [32] and etc.) and DAMA/LIBRA [33], as wall as the satellite detectors such as PAMELA [34], Planck [3,4] and others, with the necessary information on the nuclear detectors [35] and how cosmic rays moves in the Galaxy [36].…”

Section: Discussionmentioning

confidence: 99%

Unified scenario of three types of neutrinos with respective mass scales

2014

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A unified theory of including all kinds of dark matters into a single species (field) is discussed. In particular, it is considered that the Warm Dark matter (WDM), the existence of which may be required by the detailed N -body simulations of galaxies using the ΛCDM model, is the right-handed neutrino, the Hot Dark Matter (HDM) is the lefthanded neutrino, and the Cold Dark Matter (CDM) is the first KaluzaKlein (KK) mode of neutrino. The study on how to detect the first KK neutrino mode as CDM by LHC, SuperK, and IceCube is also explained. Not only these detectors but also the recent experiments, such as DAMA/LIBRA, PAMELA, XENON100, and XMASS as well as the various satellite detectors including Planck should be examined.

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Results from PAMELA, ATIC and FERMI: Pulsars or dark matter?

Cited by 8 publications

References 173 publications

Constraints on ultracompact minihalos from extragalactic γ-ray background

Constraints on ultracompact minihalos from extragalactic γ-ray background

Cosmic ray Monte Carlo: A global fitting method in studying the properties of the new sources of cosmice±excesses

Unified scenario of three types of neutrinos with respective mass scales

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